Timing observations of the binary pulsar PSR 0655 + 64

We present the results of 6.5 years of timing observations of PSR 0655 + 64 and derive an ephemeris and precise position. The very small period derivative of $$6.9 \times {10}^{-19}\,\text{s}\,{\text{s}}^{-1}$$ implies a spin-down age of $$4.5 \times {10}^{9}\,\text{yr}$$ and a magnetic field of $$1.2 \times {10}^{10}\,\text{G}$$. Kulkarni's optical identification of the companion star is confirmed. The measured eccentricity of $$7.5 \times {10}^{-6}$$ may be partly due to a general relativistic delay caused by the passage of pulses through the gravitational field of the companion star. A significant relativistic advance of the periastron should be observable over a period of ≲ 30 yr.